This study depends on KIC 9641031 eclipsing binary system with a chromospherically active component. There are three type variations, such as geometrical variations due to eclipses, sinusoidal variations due to the rotational modulations and also flares, in the light curves obtained with the data taken from the Kepler Mission Database. Taking into account results obtained from KIC 9641031's observations in the Kepler Mission Database, we present and discuss the details of chromospheric activity. The sinusoidal light variations due to rotational modulation and the flare events were modelled separately. 92 different data subsets separated using the analytic models described in the literature were modelled separately to obtain the cool spot configuration. It is seen that just one component of the system is chromospherically active star. On this component, there are two active regions separated by about 180 deg longitudinally between the latitudes of +50 deg and +100 deg, whose locations and forms are rapidly changing in short time intervals. 240 flares were detected and their parameters were computed. Using these parameters, the One Phase Exponential Association (hereafter OPEA) function model was derived, in which the Plateau value as a saturation level of the flare-equivalent duration was found to be 1.232 s for KIC 9641031, and half-life parameter was found to be 2291.7 s. The flare frequency N1 was found to be 0.41632 h-1, while the flare frequency N2 was found to be 0.00027. Considering these parameters together with the orbital period variations demonstrates that the period variations directly depend on chromospheric activity. Comparing the system with its analogue it is seen that the activity level of KIC 9641031 is remarkablely lower than the others.Comment: 26 pages, 7 figures, 4 tabel
RESUMENFavor de proporcionar un resumen en español. If you are unable to translate your abstract into Spanish, the editors will do it for you. ABSTRACTIn this study, we present the results obtained from KIC 9761199's the photometrical data acquired by the Kepler Mission. The light curve of the system, the sinusoidal variation out-of-eclipses and instant-short term flare events in the entire light curves were analyzed. The temperature of the secondary component was found to be 3891±1 K, while the mass ratio of the components (q) was found to be 0.69±0.01, and the orbital inclination (i) was computed as 77 • .4 ± 0 • .1. The sinusoidal variation is caused by the stellar spots of two active regions separated by about 180 • longitudinally located around the latitudes of +47 • and +30 • . In addition, 94 flares were detected and their parameters were computed. The OPEA model was derived for these flares and its parameters were computed. The P lateau value as saturation level for the active component was found to be 1.951±0.069 s, while the half − lif e value was found to be 1014 s. The flare frequency N 1 was found to be 0.01351 h −1 , while the flare frequency N 2 was found to be 0.00006. Maximum flare rise time (T r ) was found to be 1118.098 s, while maximum flare total time (T t ) was found to be 6767.72 s. Comparing its analogue it is seen that the chromospheric activity level of KIC 9761199, which is a low-mass close binary system according to the light curve analyses, is an expected level according to the (B − V ) color index of 1 m .303 for the active component.
We present the findings about chromospheric activity nature of KOI-256 obtained from the Kepler Mission data. Firstly, it was found that there are some sinusoidal variations out-of-eclipses due to cool spot activity. The sinusoidal variations modelled by the SPOTMODEL program indicate that the active component has two different active regions. Their longitudinal variation revealed that one of them has a migration period of 3.95 years, while the other has a migration period of 8.37 years. Secondly, 225 flares were detected from the short cadence data in total. The parameters, such as increase (Tr) and decay (T d ) times, total flare time (Tt), equivalent durations (P ), were calculated for each flare. The distribution of equivalent durations versus total flare times in logarithmic scale is modelled to find flare activity level. The P lateau value known as the saturation level of the active component was calculated to be 2.3121±0.0964 s, and the Half − lif e value, which is required flare total time to reach the saturation, was computed to be 2233.6 s. In addition, the frequency of N1, which is the number of flares per an hour in the system, was found to be 0.05087 h −1 , while the flare frequency N2 that the flare-equivalent duration emitting per an hour was found to be 0.00051. Contrary to the spot activity, it has been found that the flares are in tends to appear at specific phases due to the white dwarf component.
This study presents results obtained from the data of KIC 6044064 (KOI 6652). KIC 6044064 was observed by the Kepler Mission for a total of 1384.254 days. 525 minima times were determined, 264 of which were primary minima and the rest were secondary minima. The OPEA model was derived and its parameters were obtained. On the secondary component, there are two different spot bands latitudinally outstretched, consisting of three spots located with a phase interval of 0.33. The average migration period was found to be 623.063±4.870 days (1.71±0.01 years) for the first spot group, while it was 1125.514±7.305 days (3.08±0.02 years) for the second group. The spectral types of the components seem to be G7V+K9V. Their masses and radii were determined to be 0.86Mʘ and 0.89Rʘ for the primary component and 0.54Mʘ and 0.62Rʘ for the secondary component.
We present the findings for the magnetic activities seen on V1130 Cyg and V461 Lyr. In the case of V1130 Cyg, the secondary component's temperature was found to be 3891±50 K, while the mass ratio was computed as 0.689±0.001, and the orbital inclination as 90°.00±0°.01. The temperature of V461 Lyr's secondary component was found to be 4206±50 K, and the mass ratio was calculated as 0.999±0.001 with 89°.58±0°.01 of orbital inclination. The analyses exhibit the effects of the stellar spots on the light curves. The models indicate that there are two types of flares in the case of V1130 Cyg, and three types of flares for V461 Lyr. The Plateau parameters have been found as 2.1997 s for Group 1 and 1.0068 s for Group 2 in the case of V1130 Lyr. They have been computed as 1.9015 s for Group 1, 2.7943 s for Group 2, and 3.4324 s for Group 3 of V461 Lyr.
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